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MetadataRightsList Access
Text
Interplanetary Coronal Mass Ejections (ICMEs) from Wind and ACE Data during 1995 − 2009
ResourceID
spase://NASA/Catalog/Wind/ICME_List
Description
The ICMEs are identified based by inspection of a combination of signatures: a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a low proton temperature, a higher density ratio of alpha particles to protons, an enhancement of total perpendicular pressure (Pt), a declining solar wind speed, etc. At least three of the above features are required to identify an ICME, with careful consideration of ambient solar wind. The boundaries of ICMEs are identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties. For ambiguous events, we have checked the SOHO LASCO CME catalog and STEREO SECCHI observations. When there is a clear magnetic
obstacle (flux rope) in an ICME, we give the start time of the magnetic obstacle as well.
In order to survey the ICMEs as completely as possible, the ACE data has been used when the Wind data were unavailable or noisy and when Wind was near or within the magnetosphere.
1. Jian et al (Solar Physics, 239, 393-436, doi: 10.1007/s11207-006-0132-2, 2006) gives more details about the identification criteria and also the ICME list of 1995 – 2004.
2. The ICME list of 1995 – 2006 is an appendix of Lan Jian's 2008 PhD thesis from UCLA.
3. Jian et al. (Solar Physics, 274, 321-344, doi: 10.1007/s11207-011-9737-2, 2011) updates the results to 2009.
4. The solar cycle variation from 1995 to 2011 is published in Jian et al. (Amer. Inst. Phys. Proceedings of Solar Wind 13, 1539, 195-198, doi: 10.1063/1.4811021, 2013), where STEREO A/B is used for 1-AU observation beyond 2009.
Metadata Rights
CC0-1.0:
Creative Commons Zero v1.0 Universal
Note
CC0 1.0 Universal is the Creative Commons license applicable to all publicly available SPASE metadata descriptions. The actual data/software may be subject to a different license.
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Details
Version:2.7.1
Catalog
ResourceID
spase://NASA/Catalog/Wind/ICME_List
NamingAuthority
NASA
ResourceType
Catalog
ResourceHeader
ResourceName
Interplanetary Coronal Mass Ejections (ICMEs) from Wind and ACE Data during 1995 − 2009
ReleaseDate
2026-02-02 13:10:27Z
RevisionHistory
RevisionEvent
ReleaseDate
2025-03-20 14:37:19
Note
Only known prior ReleaseDate of the metadata
RevisionEvent
ReleaseDate
2026-02-02 13:10:27Z
Note
Added MetadataRightsList. Updated to 2.7.1. Changed http to https in top-level schemaLocation attribute. Fixed version number separator in top-level schemaLocation attribute. ZCB
Description
The ICMEs are identified based by inspection of a combination of signatures: a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a low proton temperature, a higher density ratio of alpha particles to protons, an enhancement of total perpendicular pressure (Pt), a declining solar wind speed, etc. At least three of the above features are required to identify an ICME, with careful consideration of ambient solar wind. The boundaries of ICMEs are identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties. For ambiguous events, we have checked the SOHO LASCO CME catalog and STEREO SECCHI observations. When there is a clear magnetic
obstacle (flux rope) in an ICME, we give the start time of the magnetic obstacle as well.
In order to survey the ICMEs as completely as possible, the ACE data has been used when the Wind data were unavailable or noisy and when Wind was near or within the magnetosphere.
1. Jian et al (Solar Physics, 239, 393-436, doi: 10.1007/s11207-006-0132-2, 2006) gives more details about the identification criteria and also the ICME list of 1995 – 2004.
2. The ICME list of 1995 – 2006 is an appendix of Lan Jian's 2008 PhD thesis from UCLA.
3. Jian et al. (Solar Physics, 274, 321-344, doi: 10.1007/s11207-011-9737-2, 2011) updates the results to 2009.
4. The solar cycle variation from 1995 to 2011 is published in Jian et al. (Amer. Inst. Phys. Proceedings of Solar Wind 13, 1539, 195-198, doi: 10.1063/1.4811021, 2013), where STEREO A/B is used for 1-AU observation beyond 2009.
Contacts
Role
Person
StartDate
StopDate
Note
1.
AuthorGeneralContact
spase://SMWG/Person/Lan.Jian
2.
MetadataContact
spase://SMWG/Person/Olga.Y.Uritskaya
AccessInformation
RepositoryID
spase://SMWG/Repository/ACE_SC
AccessURL
URL
https://izw1.caltech.edu/ACE/ASC/DATA/level3/ICME_List_1995_2009_Jian.pdf
Format
Text
InstrumentIDs
spase://SMWG/Instrument/ACE/MAG
spase://SMWG/Instrument/Wind/MFI
PhenomenonType
InterplanetaryCoronalMassEjection
TimeSpan
StartDate
1995-02-08 03:10:00
StopDate
2009-12-12 04:39:00
Parameter #1
Name
#
Support
SupportQuantity
Other
Parameter #2
Name
Start
Units
UT [mm/dd hhmm]
Support
SupportQuantity
Temporal
Parameter #3
Name
Start UT of Magnetic Obstacle
Units
UT [mm/dd hhmm]
Support
SupportQuantity
Temporal
Parameter #4
Name
End
Units
UT [mm/dd hhmm]
Support
SupportQuantity
Temporal
Parameter #5
Name
Discontinuity
Units
UT [mm/dd hhmm]
Support
SupportQuantity
Temporal
Parameter #6
Name
F/R Shock
Description
For most Group 3 ICMEs, the spacecraft do not traverse some part of magnetic obstacle, so that the start time of obstacle is not given for such events.
The stop time of the magnetic obstacle, not given in the survey, is the same as the end time of the ICME event.
Support
SupportQuantity
Other
Parameter #7
Name
Ptmax
Units
pPa
Support
SupportQuantity
Other
Parameter #8
Name
Vmax
Units
km/s
Support
SupportQuantity
Velocity
Parameter #9
Name
Vmin
Units
km/s
Support
SupportQuantity
Velocity
Parameter #10
Name
ΔV
Description
ΔV: change in solar wind velocity during one event; negative value indicates that the solar wind velocity declines through the event
Units
km/s
Support
SupportQuantity
Velocity
Parameter #11
Name
Bmax
Units
nT
Support
SupportQuantity
Other
Parameter #12
Name
Group
Description
Group: classification of ICME into three groups depending on the time variation of Pt.
Group 1: central maximum of Pt;
Group 2: plateau-like profile of Pt;
Group 3: gradual decrease after sharp increase at the leading edge.
From Group 1 to Group 3, the relative impact distance between spacecraft and central flux rope approximately increases.
Support
SupportQuantity
Other
Parameter #13
Name
Comments
Support
SupportQuantity
Remark